We present new Atacama Large Millimeter/sub-millimeter Array ( ALMA ) 1.3 mm continuum observations of the SR 24S transition disk with an angular resolution \lesssim 0.18 ^ { \prime \prime } ( 12 au radius ) .
We perform a multi-wavelength investigation by combining new data with previous ALMA data at 0.45 mm .
The visibilities and images of the continuum emission at the two wavelengths are well characterized by a ring-like emission .
Visibility modeling finds that the ring-like emission is narrower at longer wavelengths , in good agreement with models of dust trapping in pressure bumps , although there are complex residuals that suggest potentially asymmetric structures .
The 0.45 mm emission has a shallower profile inside the central cavity than the 1.3 mm emission .
In addition , we find that the ^ { 13 } CO and C ^ { 18 } O ( J=2-1 ) emission peaks at the center of the continuum cavity .
We do not detect either continuum or gas emission from the northern companion to this system ( SR 24N ) , which is itself a binary system .
The upper limit for the dust disk mass of SR 24N is \lesssim 0.12 M _ { \bigoplus } , which gives a disk mass ratio in dust between the two components of M _ { \mathrm { dust,SR 24 S } } / M _ { \mathrm { dust,SR 24 N } } \gtrsim 840 .
The current ALMA observations may imply that either planets have already formed in the SR 24N disk or that dust growth to mm-sizes is inhibited there and that only warm gas , as seen by ro-vibrational CO emission inside the truncation radii of the binary , is present .